  We investigate the present distributions of gas and young stars in the Large
and Small Magellanic Clouds (LMC and SMC) based on fully self-consistent
numerical simulations of the Clouds for the last ~ 0.8 Gyr. Our principal
results, which can be tested against observations, are as follows. The last
dynamical and hydrodynamical interaction between the Clouds about ~ 0.2 Gyr ago
can form the apparently off-center bar and peculiar HI spirals of the LMC. The
present spatial distributions of young stars with ages less than 20 Myr in the
LMC can be significantly asymmetric and clumpy owing to the interaction. A
small but non-negligible fraction of stellar and gaseous components can be
transferred from the SMC into the LMC during the interaction to form diffuse
halo components around the LMC. The burst of star formation in the SMC can be
synchronized with that of the LMC about 0.2 Gyr ago in some models. New stars
can form from gas in the SMC's tidal tails, one of which can be observed as the
Magellanic Bridge (MB). The metallicity distribution function of new stars in
the MB has a peak of [Fe/H] ~ -0.8, which is significantly smaller than the
stellar metallicity of the SMC. Based on these results, we discuss the origin
of 30 Doradus, the southern molecular ridge of the LMC, the globular cluster
ESO 121-SC03, metal-poor inter-Cloud stars within the MB, and giant HI holes of
the LMC.
