  Probing statistical distribution of the neutral hydrogen (\HI) using the
redshifted 21-cm hyperfine-transition spectral line holds the key to understand
the formation and evolution of the matter density in the universe. The
two-point statistics of the \HI distribution can be estimated by measuring the
power spectrum of the redshifted 21-cm signal using visibility correlation. A
major challenge in this regard is that the expected signal is weak compared to
the foreground contribution from the Galactic synchrotron emission and
extragalactic point sources in the observing frequencies. In this work, we
investigate the possibility of detecting the power spectrum of the redshifted
21-cm signal by using strong gravitational lensing of the galaxy clusters. This
method has the advantage that it only enhances the \HI signal and not the
diffuse galactic foreground. Based on four simple models of the cluster
potentials we show that the strong lenses at relatively lower redshifts with
more than one dark matter halo significantly enhances the 21-cm signal from the
post reionization era. We discuss the merits and demerits of the method and the
future studies required for further investigations.
