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We investigate the production of non-thermal dark matter (DM), $\chi$, duringpost-inflationary reheating era. For the inflation, we consider two slow rollsingle field inflationary scenarios - generalized version of Hilltop (GH)inflation, and Coleman-Weinberg (NM-CW) inflation with non-minimal couplingbetween inflaton and curvature scalar. Using a set of benchmark values thatcomply with the current constraints from Cosmic Microwave Background Radiation(CMBR) data for each inflationary model, we explored the parameter spaceinvolving mass of dark matter particles, $m_\chi$, and coupling betweeninflaton and $\chi$, $y_\chi$. For these benchmarks, we find thattensor-to-scalar ratio $r$ can be as small as $2.69\times 10^{-6}$ for GH and$3\times 10^{-3}$ for NM-CW inflation, both well inside $1-\sigma$ contour onscalar spectral index versus $r$ plane from Planck 2018+BICEP 3+Keck Array 2018dataset, and testable by future cosmic microwave background (CMB) observationse.g. Simons Observatory. For the production of $\chi$ from the inflaton decaysatisfying CMB and other cosmological bounds and successfully explaining totalcold dark matter density of the present universe, we find that $y_\chi$ shouldbe within this range ${\cal O}\left(10^{-8}\right) \gtrsim y_\chi\gtrsim {\calO}\left(10^{-17}\right)$ for both inflationary scenarios. We also show that,even for the same inflationary scenario, the allowed parameter space onreheating temperature versus $m_\chi$ plane alters with inflationary parametersincluding scalar spectral index, tensor-to-scalar ratio, and energy scale ofinflation.

Post-inflationary production of particle Dark Matter: Hilltop and Coleman-Weinberg inflation