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We study the evolution of three fields in the outer LMC disk Rgc=3.5-6.2 Kpc.Their star formation history indicates a stellar populations gradient such thatyounger stellar populations are more centrally concentrated. We identify twomain star forming epochs, separated by a period of lower activity between ~7and ~4 Gyr ago. Their relative importance varies from a similar amount of starsformed in the two epochs in the innermost field, to only 40% of the starsformed in the more recent epoch in the outermost field. The young star formingepoch continues to the present time in the innermost field, but lasted onlytill ~0.8 and 1.3 Gyr ago at Rgc=5.5 degrees and 7.1 degrees, respectively.This gradient is correlated with the measured HI column density and implies anoutside-in quenching of the star formation, possibly related to a variation ofthe size of the HI disk. This could either result from gas depletion due tostar formation or ram-pressure stripping, or from to the compression of the gasdisk as ram-pressure from the Milky Way halo acted on the LMC interstellarmedium. The latter two situations may have occurred when the LMC firstapproached the Milky Way.

Spatially resolved LMC star formation history: I. Outside in evolution of the outer LMC disk