  We first show that a large amount of metal-poor gas is stripped from the
Small Magellanic Cloud (SMC) and fallen into the Large Magellanic Cloud (LMC)
during the tidal interaction between the SMC, the LMC, and the Galaxy over the
last 2 Gyrs. We propose that this metal-poor gas can closely be associated with
the origin of LMC's young and intermediate-age stars and star clusters with
distinctively low-metallicities with [Fe/H] < -0.6. We numerically investigate
whether gas initially in the outer part of the SMC's gas disk can be stripped
during the LMC-SMC-Galaxy interaction and consequently can pass through the
central region (R<7.5 kpc) of the LMC. We find that about 0.7 % and 18 % of the
SMC's gas can pass through the central region of the LMC about 1.3 Gyr ago and
0.2 Gyr ago, respectively. The possible mean metallicity of the replenished gas
from the SMC to LMC is about [Fe/H] = -0.9 to -1.0 for the two interacting
phases. These results imply that the LMC can temporarily replenish gas supplies
through the sporadic accretion and infall of metal-poor gas from the SMC. These
furthermore imply that if these gas from the SMC can collide with gas in the
LMC to form new stars in the LMC, the metallicities of the stars can be
significantly lower than those of stars formed from gas initially within the
LMC.
