  We present nine color CCD intermediate-band spectrophotometry of a two square
degree field centered on the old open cluster M67, from 3890$\rm \AA$ to nearly
1$\mu$. These observations are taken as a part of the BATC
(Beijing-Arizona-Taipei-Connecticut) Color Survey of the Sky, for both
scientific and calibration reasons. With these data we show that the BATC
survey can reach its goal of obtaining spectrophotometry to a zero point
accuracy of 0.01 mag, and down to V = 21 with 0.3 mag random error. We fit the
color-magnitude diagrams (CMDs) with Worthey's theoretical models. The net
result is the excellent fit of the 4.0 Gyr, [Fe/H] = $-0.10$ model to our data,
including a good fit to the main sequence (MS) turn-off. Our data are
consistent with a toy model with 50\% of the stars in M67 being binaries and a
random distribution of binary mass-ratios, although other models with different
mass-ratio distributions cannot be ruled out. The spatial distribution and mass
function (MF) of stars in M67 show marked effects of dynamical evolution and
evaporation of stars from the cluster. Blue stragglers and binary stars are the
most condensed within the cluster, with degree of condensation depending on
mass.We find M67 to have an elongated shape, oriented at an angle of
$15^{\circ}$ relative to the galactic plane. Within its tidal radius, the
observed MF of M67 between 1.2 $\rm M_\odot$ and $\rm 0.8 M_\odot$ has a
Salpeter slope $\rm \eta = -1.93 \pm 0.66$. For stars of mass below 0.8 $\rm
M_\odot$, $\rm \eta \sim 0$. It is plausible that the leveling-off of the MF at
lower masses is a result of evaporation of lower mass stars in this mass range
at a rate of one every $\sim 10^7$ years. If so, it is plausible that the IMF
of M67 has the canonical field value of $\rm \eta = -2.0$.
