This paper presents the calibration ofTully-Fisher relations based on Cepheid distances BV RIH~0 .5 to 21 galaxies within 25 Mpc and 23 clusters within 10,000 km s~1. These relations have been applied to several distant cluster surveys in order to derive a value for the Hubble constant, mainly concentrat-H 0 , ing on an I-band all-sky survey by Giovanelli and collaborators, consisting of total I magnitudes and 50% line width data for D550 galaxies in 16 clusters. For comparison, we also derive the values of H 0 using surveys in the B and V bands by Bothun and collaborators, and in H band by Aaronson and collaborators. Careful comparisons with various other databases from the literature suggest that the H-band data, which have isophotal magnitudes extrapolated from aperture magnitudes rather than total magnitudes, are subject to systematic uncertainties. Taking a weighted average of the estimates of Hubble constants from four surveys, we obtain (random)^7 (systematic). We have also H 0 \ 71^4 investigated how the value of is a †ected by various systematic uncertainties, such as the internal H 0 extinction correction method used, Tully-Fisher slopes and shapes, a possible metallicity dependence of the Cepheid period-luminosity relation, and cluster population incompleteness bias.