Primordial Black Holes and Gravitational Waves in Hybrid Inflation with
  Chaotic Potentials
  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. A wide mass range of PBH is
realized in our models, and the frequencies of scalar induced gravitational
waves are ranged from nHz to Hz. 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 space-based gravitational wave (GW)
observatories. The formation of $~10 \, M_{\odot}$ PBH with wide peaks of SIGWs
can be used to interpret the stochastic GW signal in the nHz band, detected by
the North American Nano hertz Observatory (NANO-Grav) for Gravitational Waves.
These signals may also be tested by future interferometer-type GW observations
of EPTA, SKA, LISA, TaiJi, TianQin and Einstein Telescope (ET).
