  The main objective of this manuscript is to investigate the bouncing
cosmology in the background of $f(\mathcal{Q})$ gravity, where $\mathcal{Q}$
defines the non-metricity. For this purpose, we use the reconstruction approach
and consider a flat Friedmann-Robertson-Walker spacetime with perfect matter
configuration. We examine how the first contracting phase gives the expansion
by using a temporal derivative of the scale factor, i.e., $\dot{a}<0$,
$\dot{a}=0$ and $\dot{a}>0$ give contraction, bounce point and expansion
phases, respectively. Further, we use the order reduction method to solve the
modified field equations as these are very difficult due to the presence of
additional non-linear expressions. It is analyzed that the original singularity
of the universe diminishes for the required bounce conditions. We conclude that
the acceleration occurs near the bouncing point and the considered
$f(\mathcal{Q})$ models are consistent with the current cosmic accelerated
expansion.
