  We present the results of a Chandra/HST study of the point sources of the NGC
4472. We identify 144 X-ray sources, 72 with HST matches. The optical data show
1102 sources, 829 with globular cluster colors. Thirty matches are found -
likely to be low mass X-ray binaries in globular clusters, while 42 have no
optical counterparts to V~25 and I~24 - likely predominantly LMXBs in the field
star population. Thus approximately 40% of the X-ray sources are in globular
clusters and ~4% of the globular clusters contain X-ray sources. The blue GC
sources may have harder X-ray spectra than the red GC sources. No significant
differences are found between the X-ray properties of the field sources and of
the GC sources. This study, along with our previous result from Paper I in this
series on the similarity of the spatial profile of the field LMXBs, globular
cluster LMXBs, and the globular clusters themselves suggest that a significant
fraction of the observed low mass X-ray binaries in the field may be created in
a globular cluster then ejected into the field by stellar interaction s;
however, by comparing the results for NGC 4472 with those in several other
galaxies, we find tentative evidence for a correlation be tween the globular
cluster specific frequency and the fraction of LMXBs in globular clusters, a
correlation which would be most easily explained if some of the field sources
were generated in situ. We show that isolated accreting very massive black
holes are unlikely to be observable with current X-ray instrumentation and that
these sources hence do not contaminate the LMXB population. We discuss the
possibility that several equatorial point sources may indicate the presence of
a disk wind responsible for the low radiative efficiency observed in the
nucleus of this source. (abridged)
