  We investigate the properties of massive, dense clouds formed in a barred
galaxy and their possible relation to star formation, performing a
two-dimensional hydrodynamical simulation with the gravitational potential
obtained from the 2Mass data from the barred spiral galaxy, M83. Since the
environment for cloud formation and evolution in the bar region is expected to
be different from that in the spiral arm region, barred galaxies are a good
target to study the environmental effects on cloud formation and the subsequent
star formation. Our simulation uses for an initial 80 Myr an isothermal flow of
non-self gravitating gas in the barred potential, then including radiative
cooling, heating and self-gravitation of the gas for the next 40 Myr, during
which dense clumps are formed. We identify many cold, dense gas clumps for
which the mass is more than $10^4M_{\odot}$ (a value corresponding to the
molecular clouds) and study the physical properties of these clumps. The
relation of the velocity dispersion of the identified clump's internal motion
with the clump size is similar to that observed in the molecular clouds of our
Galaxy. We find that the virial parameters for clumps in the bar region are
larger than that in the spiral arm region. From our numerical results, we
estimate star formation in the bar and spiral arm regions by applying the
simple model of Krumholtz and McKee (2005). The mean relation between star
formation rate and gas surface density agrees well with the observed
Kennicutt-Schmidt relation. The SFE in the bar region is $\sim 60 %$ of the
spiral arm region. This trend is consistent with observations of barred
galaxies.
