We present results of optical identiÐcation of the X-ray sources detected in the ASCA Large Sky Survey. Optical spectroscopic observations were done for 34 X-ray sources that were detected with the SIS in the 2È7 keV band above 3.5 p. The Ñux limit corresponds to D1 ] 10~13 ergs cm~2 s~1 in the 2È10 keV band. The sources are identiÐed with 30 active galactic nuclei (AGNs), two clusters of galaxies, and one Galactic star. Only one source is still unidentiÐed.All of the X-ray sources that have a hard X-ray spectrum with an apparent photon index of smaller than 1 in the 0.7È10 keV band are identiÐed with narrow-line or weak-broad-line AGNs at redshifts smaller than 0.5. This fact supports the idea that absorbed X-ray spectra of narrow-line and weak-broadline AGNs make the cosmic X-ray background (CXB) spectrum harder in the hard X-ray band than that of a broad-line AGN, which is the main contributor in the soft X-ray band. Assuming their intrinsic spectra are same as a broad-line AGN (a power-law model with a photon index of 1.7), their X-ray spectra are Ðtted with hydrogen column densities of at the objectÏs redshift. On log N H (cm~2) \ 22È23 the other hand, X-ray spectra of the other AGNs are consistent with that of a nearby type 1 Seyfert galaxy. In the sample, four high-redshift luminous broad-line AGNs show a hard X-ray spectrum with an apparent photon index of 1.3^0.3. The hardness may be explained by the reÑection component of a type 1 Seyfert galaxy. The hard X-ray spectra may also be explained by absorption with at the objectÏs redshift, if we assume an intrinsic photon index of 1.7. The origin log N H (cm~2) \ 22È23 of the hardness is not clear yet.Based on the log NÈlog S relations of each population, contributions to the CXB in the 2È10 keV band are estimated to be 9% for less-absorbed AGNs including the four high-(log N H (cm~2) \ 22) redshift broad-line AGNs with a hard X-ray spectrum, 4% for absorbed AGNs (22 \ log N H (cm~2) \ 23, without the four hard broad-line AGNs), and 1% for clusters of galaxies in the Ñux range from 3 ] 10~11 ergs cm~2 s~1 to 2 ] 10~13 ergs cm~2 s~1. If the four hard broad-line AGNs are included in the absorbed AGNs, the contribution of the absorbed AGNs to the CXB is estimated to be 6%.In optical spectra, there is no high-redshift luminous cousin of a narrow-line AGN in our sample. The redshift distribution of the absorbed AGNs is limited below z \ 0.5 excluding the four hard broad-line AGNs, in contrast to the existence of 15 less-absorbed AGNs above z \ 0.5. The redshift distribution of the absorbed AGNs suggests a deÐciency of AGNs with column densities of in log N H (cm~2) \ 22È23 the redshift range 0.5È2, or in the X-ray luminosity range larger than 1044 ergs s~1, or both. If the large column densities of the four hard broad-line AGNs are real, they could complement the deÐciency of X-ray absorbed luminous high-redshift AGNs.