  Here, we study the distribution of Fundamental-mode Cepheids in the
Magellanic Cloud as a function of their positions and ages using the data from
the OGLE~IV survey. Age of the Cepheids are determined through well known
period - age relations for the LMC and SMC Cepheids which are used to
understand the star formation scenario in the Magellanic Cloud. The age
distributions of the Cepheids in LMC and SMC show peak around $155^{+45}_{-35}$
Myr and $224^{+51}_{-42}$ Myr, respectively. This indicates that a major star
formation event took place in the Magellanic Cloud at about 200\,Myr ago. It is
believed that this event might have been triggered by a close encounter between
the two components of the Magellanic Cloud or due to a possible tidal
interaction between the Magellanic Cloud and Milky Way galaxy during one of its
pericentric passages round the Milky Way. Cepheids are found to be
asymmetrically distributed in both the LMC and SMC. A high-density clumpy
structure is found to be located towards eastern side of the LMC and south-west
direction of the SMC from their respective galactic centres.
