A deep imaging survey covering the entire 23' diameter of the old open cluster M67 toV=25 has been carried out using the mosaic imager (UHCam) on the Canada-France-Hawaii Telescope. The cluster color-magnitude diagram (CMD) can be traced from stars on its giant branch atM_V=+1 down through main-sequence stars at least as faint asM_V=13.5. Stars this low in luminosity have masses below 0.15M_☉. A modest white dwarf (WD) cooling sequence is also observed commencing slightly fainter thanM_V=10 and, after correction for background galaxy and stellar field contamination, terminating nearM_V=14.6. The observed WDs follow quite closely a theoretical cooling sequence for 0.7M_☉ pure carbon core WDs with hydrogen-rich atmospheres (DA WDs). The cooling time to anM_V of 14.6 for such WDs is 4.3 Gyr, which we take as the WD cooling age of the cluster. A fit of a set of isochrones to the cluster CMD indicates a turnoff age of 4.0 Gyr. The excellent agreement between these results suggests that ages derived from white dwarf cooling should be considered as reliable as those from other dating techniques. The WDs currently contribute about 9% of the total cluster mass, but the number seen appears to be somewhat low when compared with the number of giants observed in the cluster.