We have analyzed images of point-like X-ray sources obtained at the X-ray Calibration Facility (XRCF) in Huntsville, AL during the Phase H calibration period April 18-26, 1997. We describe the PRF using several methods, including the encircled energy radius, azimuthally averaged radial surface brightness profiles, radial surface brightness profiles in orthogonal, one pixel wide slices, and marginal surface brightness distributions. These spot profiles are often presented as a function of event grade distribution, which is particularly sensitive to photon event pileup. To assess and validate the Chandra telescope model, we performed identical analyses of SAOSAC+MARX simulations for several XRCF tests, and compared the results of the models directly to the XRCF data. The model included the effects of gravity, finite source distance, mirror misalignments, and the ~10% decrease in the mirror effective area discovered during the HRMA Phase F calibration. The model included the additional effects of finite source size for the on-axis PRF core measurement, but did not account for non-monochromaticity of the X-ray source. The ACIS+HRMA point response function (PRF) shows a complex dependence on the incident count rate, defocus, pixel size, detector geometry, and most importantly the HRMA (mirror) properties. The model is sharper than the XRCF on-axis data by ~7% in the on axis FWHM and ~3% in the 70% encircled energy radius. The accuracy of this comparison is limited by unmodeled CCD pixelation effects. The off-axis model spot beyond four arcminutes is sharper in the 70% encircled energy radius compared to the XRCF spot by only ~<10%, and the rate of growth of the model and XRCF spots with increasing off-axis angle agree to within the measurement errors. This Memorandum is intended as a brief summary of the detailed analyses and data products available on the web at http://asc.harvard.edu/cal/Links/Acis/acis/Cal_prods/psf/psf.html.