  We investigate the production of non-thermal fermionic dark matter particles
during the reheating era following slow roll inflation, driven by axion-like
pseudo-Nambu-Goldstone boson, $\varphi$, that is non-minimally coupled to the
curvature scalar, ${\cal R}$. We consider two types of non-minimal coupling,
one of which is $\xi \varphi^2 {\cal R}$ (referred to as NM-N), and the other
one is $\alpha\left( 1+ \cos\left(\frac{\varphi}{f_a}\right)\right)$ (referred
to as NMP-N), where $\alpha$ and $\xi$ are dimensionless parameters and $f_a$
is an energy scale. We determine benchmark values for both inflationary
scenarios satisfying current bounds from Cosmic Microwave Background (CMB)
radiation measurement and find the mass of inflaton to be $\sim {\cal
O}\left(10^{12}\right) \text{GeV}$ for both inflationary scenarios and
tensor-to-scalar ratio, $r\sim 0.0177$ (for NM-N) and $\sim 0.0097$ (for NMP-N)
which fall inside $1-\sigma$ contour on scalar spectral index versus $r$ plane
of Planck 2018+Bicep 3+Keck Array 2018 joint analysis, and can be probed by
future CMB observations e.g. Simons Observatory. We then show that dark matter
particles produced from the decay of inflaton can fully match the present-day
cold dark matter (CDM) yield, as well as other cosmological constraints, if the
coupling value between inflaton and dark matter, $y_\chi$, and the dark matter
mass, $m_\chi$, are within the range $10^{-6}\gtrsim y_\chi\gtrsim 10^{-17}$
and ${\cal O}(1\text{GeV})\lesssim m_\chi\lesssim m_\phi/2$, where $m_\phi$
denotes the mass of inflaton. The exact range of $y_\chi$ and $m_\chi$ varies
with different benchmark values as well as parameters of inflation, like energy
scale of inflation and $r$, some of which are within the reach of next
generation CMB experiments.
