  Recent studies have shown that an extended main-sequence turn-off is a common
feature among intermediate-age clusters (1--3 Gyr) in the Magellanic Clouds.
Multiple-generation star formation and stellar rotation or interacting binaries
have been proposed to explain the feature. However, it remains controversial in
the field of stellar populations. Here we present the main results of an
ongoing star formation among older star clusters in the Large Magellanic Cloud.
Cross-matching the positions of star clusters and young stellar objects has
yielded 15 matches with 7 located in the cluster center. We demonstrate that
this is not by chance by estimating local number densities of young stellar
objects for each star cluster. This method is not based on isochrone fitting,
which leads to some uncertainties in age estimation and methods of background
subtraction. We also find no direct correlation between atomic hydrogen and the
clusters. This suggests that gas accretion for fueling the star formation must
be happening in situ. These findings support for the multiple-generations
scenario as a plausible explanation for the extended main-sequence turn-off.
