  We have analyzed the low mass X-ray binary (LMXB) candidates in a Chandra
observation of the giant elliptical galaxy NGC 4472. In a region observed by
the Hubble Space Telescope, approximately 40% of the bright (L_X >= 10^37
ergs/s) LMXBs are associated with optically identified globular clusters (GC).
This is significantly higher than the fraction of bright LMXBs in Galactic GCs
and confirms that GCs are the dominant sites of LMXB formation in early type
galaxies. The approximately 4% of NGC 4472 GCs hosting bright LMXBs, on the
other hand, is remarkably similar to the fraction of GCs with LMXBs in every
other galaxy. Although statistical tests suggest that the luminosity of a
cluster is an important driver of LMXB formation in GCs, this appears largely
to be a consequence of the greater number of stars in bright clusters. The
metallicity of GCs is a strong determinant of LMXB specific frequency, with
metal-rich clusters about 3 times more likely to host LMXBs than metal-poor
ones. There are weaker dependences on the size of a GC and its distance from
the center of the galaxy. The X-ray luminosity does not depend significantly on
the properties of the host GC. Furthermore, the spatial distribution and X-ray
luminosity function of LMXBs within and outside GCs are indistinguishable. The
X-ray luminosity function of both GC-LMXBs and non-GC-LMXBs reveal a break at
approximately 3x10^38 ergs/s strongly suggesting that the brightest LMXBs are
black hole accretors.
