  We present high resolution (~2.5'') CO(1-0) and CO(2-1) images of the central
kiloparsec of NGC 3077 made with the Owens Valley Millimeter Array. CO emission
is distributed in three major complexes which resolve into at least seven GMCs.
Two complexes are associated with the central starburst. A third, more distant
complex is not associated with strong star formation. The GMCs are ~70 pc in
size and contain ~10^{6} M_{\odot} of molecular gas. The Galactic conversion
factor appears applicable to NGC 3077, consistent with its solar metallicity.
Galactic rotation in NGC 3077 is detected for the first time in the molecular
gas. The molecular gas counterrotates with respect to the large scale HI tidal
bridge. The molecular clouds closest to the starburst have super-virial
linewidths, possibly related to the turbulence generated by the starburst. The
2.6 mm radio continuum flux indicates that thermal Bremsstrahlung dominates the
emission from the starburst region below 5 cm, and that the N_{Lyc} \simeq
3.7\times 10^{52} s^{-1} or ~3000 O7 stars, corresponds to a star formation
rate of 0.4 M_{\odot} yr^{-1}. At this rate the amount of molecular gas can
sustain star formation for only ~10 Myrs; thus NGC 3077 is a true starburst
galaxy. The derived age of the starburst is consistent with the inferred ages
of the superbubbles, which suggests that the burst is much younger than the age
of the M 81-M 82-NGC 3077 interaction. We suggest that it is caused by gas that
was pulled out of NGC 3077 during the interaction with M 81, raining back down
onto the galaxy.
