  From the analysis of the color-magnitude diagrams and color functions of four
wide LMC fields located from ~2 to 6 kpc from the kinematic center of the LMC
we present evidence that, while the oldest population is coeval in all fields,
the age of the youngest component of the dominant stellar population gradually
increases with galactocentric distance, from currently active star formation in
a field at 2.3 deg, to 100 Myr, 0.8 Gyr, and 1.5 Gyr in fields at 4.0 deg, 5.5
deg, and 7.1 deg, respectively. This outside-in quenching of the star formation
in the LMC disk is correlated with the decreasing HI column density (which is <
2x 10^{20} cm^{-2} in the two outermost fields with little or no current star
formation. Other work in the literature hints at similar behavior in the
stellar populations of irregular galaxies, and in M33. This is observational
evidence against the inside-out disk formation scenario in low-mass spirals and
irregular galaxies. Alternatively, it could be that the age distribution with
radius results from interplay between the evolution with time of the
star-forming area of the LMC and the subsequent outward migration of the stars.
