  We perform a 2.5 dimensional magnetohydrodynamic (MHD) simulation to
understand a comprehensive view of the formation of spicule-like cool jets due
to initial transverse velocity pulses akin to Alfv\'en pulses in the solar
chromosphere. We invoke multiple velocity ($V_{z}$) pulses between 1.5 and 2.0
Mm in the solar atmosphere, which create the initial transverse velocity
perturbations. These pulses transfer energy non-linearly to the field aligned
perturbations due to the ponderomotive force. This physical process further
creates the magnetoacoustic shocks followed by quasi-periodic plasma motions in
the solar atmosphere. The field aligned magnetoacoustic shocks move upward
which subsequently cause quasi-periodic rise and fall of the chromospheric
plasma into the overlying corona as a thin and cool spicule-like jets. The
magnitude of the initial applied transverse velocity pulses are taken in the
range of 50-90 km $s^{-1}$. These pulses are found to be strong enough to
generate the spicule-like jets. We analyze the evolution, kinematics and
energetics of these spicule-like jets. We find that the transported mass flux
and kinetic energy density are substantial in the localized solar-corona. These
mass motions generate $\it in$ $situ$ quasi-periodic oscillations on the scale
of $\simeq$ 4.0 min above the transition region.
