  We survey globular clusters (GCs) in M85 using $ugi$-band images of a
$1^{\circ} \times 1^{\circ}$ field obtained with the MegaCam at the 3.6 m
Canada-France-Hawaii Telescope. We identify 1318 GC candidates with 20.0 mag $<
g_0 <$ 23.5 mag in the entire survey region. Their radial number density
profile is well fit by a S{\'e}rsic profile with $n$ = 2.58$^{+0.43}_{-0.33}$
and effective radius $R_{\rm e,GCS}$ = 4$\rlap{.}{'}$14 (= 22 kpc), showing
that the candidates at $R < 20'$ are mostly genuine GCs in M85. We estimate the
total number of GCs, $N$(total) = $1216^{+82}_{-50}$, and the specific
frequency, $S_N = 1.41^{+0.10}_{-0.06}$. The overall color distribution of the
GCs in M85 is bimodal, but the GCs in the central region at $R < 2'$ do not
show a bimodal distribution clearly. The radial number density profile and
surface number density map of the blue GCs (BGCs) show more extended structures
than those of the red GCs (RGCs). The spatial distributions of both BGCs and
RGCs are elongated, similar to that of the galaxy stellar light. The number
fraction of the RGCs in the central region is much smaller compared to those in
other early-type galaxies of similar luminosity. The mean $(g-i)_0$ color of
the RGCs in M85 is about 0.1 mag bluer than typical values for other Virgo
early-type galaxies of similar luminosity, indicating that a significant
fraction of the RGCs in M85 may be younger than typical GCs. These results
indicate that M85 might have undergone a major wet merger recently.
