  The galactic tidal interaction is a possible mechanism to trigger the active
star formation in galaxies. Recent analyses using the Hi data in the Large
Magellanic Cloud (LMC) proposed that the tidally driven colliding HI flows,
induced by the galactic interaction with the Small Magellanic Cloud (SMC),
triggered high-mass star formation in the southeastern HI Ridge, including R136
and $\sim$400 O/WR stars, and the galactic center region hosting the N44
region. This study performed a comprehensive HI data analysis across the LMC
and found that two Hi velocity components defined in the early studies (L- and
D- components) are quasi-ubiquitous with signatures of interaction dynamically
toward the other prominent HII regions, such as N11 and N79. We characterize
the intimidate velocity range (I-component) between the two components as the
decelerated gas by momentum conservation in the collisional interaction. The
spatial distributions of the I-component and those of the O/WR stars have good
agreements with each other whose fraction is more than $\sim$70% at a scale of
$\sim$15 pc, which is significantly smaller than the typical GMC size. Based on
the results of our new simulations of the LMC-SMC interaction, we propose that
the interaction about 0.2 Gyr ago induced efficient infall of gas from the SMC
to the LMC and consequently ended up with recent formation of high-mass stars
due to collisions of HI gas in the LMC. The new numerical simulations of the
gas dynamics successfully reproduce the current distribution of the
L-component. This lends theoretical support for the present picture.
