  We present results of age determination based on the standard procedure of
isochrone fitting for about 600 star clusters younger than about 1.2 Gyr from
the central parts of the LMC. Comparison of age distributions of star clusters
from the LMC and the SMC shows that cluster formation histories are different
in these galaxies. The age distribution of the LMC clusters reveals bursty
nature of cluster formation in this galaxy, with contrast to the relatively
uniform distribution of cluster ages in the SMC. We detected three extended
peaks in the distribution of ages of LMC clusters, located at about 7 Myr, 125
Myr and 0.8 Gyr. All detected peaks have complex structure. While the structure
of the youngest and the oldest peaks may be spurious due to accuracy of age
determination, in the middle peak two evident sub-peaks at 100 Myr and 160 Myr
are clearly seen. Similar peaks are seen in the distribution of ages of
clusters from the SMC, which indicates that increased cluster formation ratio
during these periods might be caused by the last encounter between the
Magellanic Clouds. The sample of clusters from the LMC is overabundant in very
young (<10 Myr) and old (>400 Myr) clusters, and underabundant in clusters
having ages in the range from 80 to 15 Myr with respect to the studied sample
of clusters from the SMC.
