  We study the formation of primordial black hole (PBH) dark matter and the
generation of scalar induced secondary gravitational waves (SIGWs) in a
non-supersymmetric model of hybrid inflation with chaotic (polynomial-like)
potential, including one-loop radiative corrections. A radiatively corrected
version of these models is entirely consistent with Planck's data. By adding
non-canonical kinetic energy term in the lagrangian, the inflaton experiences a
period of ultra-slow-roll, and the amplitude of primordial power spectrum is
enhanced to $O(10^{-2})$. The enhanced power spectra of primordial curvature
perturbations can have both sharp and broad peaks. %In the enhancement
mechanism we explore two possible extensions by employing a Guassian and a step
size kinetic function. A wide mass range of PBHs is realized in our model with
the frequencies of scalar induced gravitational waves ranged from nHz to kHz.
We present several benchmark points where the PBH mass generated during
inflation is around $(1 - 100) \, M_{\odot}$, $(10^{-9} - 10^{-7}) \,
M_{\odot}$ and $(10^{-16} - 10^{-11}) \, M_{\odot}$. The PBHs can make up most
of the dark matter with masses around $(10^{-16} - 10^{-11}) \, M_{\odot}$ and
$(1 - 100) \, M_{\odot}$, and their associated SIGWs can be probed by the
upcoming ground and space-based gravitational wave (GW) observatories. The
evidence of stochastic process recently reported by NANOGrav may be interpreted
as SIGWs associated with the formation of PBHs. These SIGWs may also be tested
by future interferometer-type GW observations of SKA, DECIGO, LISA, BBO, TaiJi,
TianQin, CE and ET.
