  CO emission has been imaged at 2" resolution in the central 10 kpc of the
barred spiral galaxy NGC 3367. This galaxy has bipolar synchrotron lobes out to
a radii of 6 kpc, straddling the compact nucleus. The peak molecular emission
is in a source of radius 2" (425 pc) centered on the galaxy nucleus. The
molecular mass is about 3 times 10**8 Msun in this peak an about 5.9 times
10**8 Msun within a radius of 4".5 (950 pc). The very large gas masses in the
central source imply extinctions sufficiently high to completely obscure
optical emission lines (e.g.BLR) associated with the nuclear radio source. The
observed Balmer lines probably originate in the narrow line region few hundred
pc from the nucleus. The CO emission in the central region is elongated NE-SW,
very similar to the PA of the large scale synchrotron lobes. This elongation is
likely due to non-axisymmetric gravitational potential of the stellar bar. We
infer that the NE radio continuum lobe is on the far side of the galaxy and the
SW lobe is on the near side. The central mass of molecular gas is sufficient
mass to power the AGN accretion luminosity for over 10**8 yrs at 3 Msun per yr.
