  We present a study of globular clusters in the inner region of the giant
elliptical galaxy NGC 4472, based on the HST WFPC2 archive data. We have found
about 1560 globular cluster candidates at the galactocentric radius r < 4
arcmin. V-(V-I) diagram of these objects shows a dominant vertical structure
which consists obviously of two components: blue globular clusters (BGCs) and
red globular clusters (RGCs). The luminosity function of the globular clusters
is derived to have a peak at V(max)=23.50+/-0.16 from Gaussian fitting. The
distance to NGC 4472 is estimated to be d=14.7+/-1.3 Mpc.The peak luminosity
for the RGCs is similar to that for the BGCs, which indicates that the RGCs may
be several Gyrs younger than the BGCs. The mean luminosity of the bright BGCs
decreases by 0.2 mag with increasing galactocentric radius over the range of 9
arcmin, while that of the RGCs does not. The observed color distribution of
these globular clusters is distinctively bimodal with peaks at (V-I) = 0.98 and
1.23. The mean observed color of all the globular clusters with V < 23.9 mag is
derived to be (V-I)=1.11. These colors are exactly the same as those for the
globular clusters in M87. It is found that the relative number of the BGCs to
the RGCs is increasing with the increasing galactocentric radius. Surface
number density profiles of both the BGCs and RGCs get flat in the central
region, and the core radii of the globular cluster systems are measured to be
r_c = 1.9 arcmin for the BGCs, r_c = 1.2 arcmin for the RGCs, and r_c = 1.3
arcmin for the total sample, which are much larger than the stellar core of the
galaxy. In general the properties of the globular clusters in the inner region
of NGC 4472 are consistent with those of the globular clusters in the outer
region of NGC 4472.
