It is not yet fully understood how planet formation affects the properties of host stars, in or out of a cluster; however, abundance trends can help us understand these processes. We present a detailed chemical abundance analysis of six stars in Praesepe, a planet-hosting open cluster. Pr0201 is known to host a close-in (period of 4.4 days) giant planet (mass of 0.54M J ), while the other five cluster members in our sample (Pr0133, Pr0081, Pr0208, Pr0051, and Pr0076) have no detected planets according to RV measurements. Using high-resolution, high signalto-noise echelle spectra obtained with Keck/HIRES and a novel approach to equivalent width measurements (XSpect-EW), we derived abundances of up to 20 elements spanning a range of condensation temperatures (T C ). We find a mean cluster metallicity of [Fe/H] = +0.21±0.02 dex, in agreement with most previous determinations. We find most of our elements show a [X/Fe] scatter of ∼0.02-0.03 dex and conclude that our stellar sample is chemically homogeneous. The T C slope for the cluster mean abundances is consistent with zero and none of the stars in our sample exhibit individually a statistically significant T C slope. Using a planet engulfment model, we find that the planet-host, Pr0201, shows no evidence of significant enrichment in its refractory elements when compared to the cluster mean that would be consistent with a planetary accretion scenario.