  We propose an inflationary scenario where the inflaton field is non-minimally
coupled to spacetime curvature and inflation is driven by a vacuum energy
symmetry breaking potential without specifying \emph{a priori} whether the
inflaton field is small or large. As we incorporate vacuum energy into our
analysis, we further explore the implications of a non-zero potential offset in
relation to the emergence of inflationary dynamics. Thus, we propose that
vacuum energy can transform into particles as a result of the transition
triggered by spontaneous symmetry breaking. This entails a vacuum energy
cancellation that yields an effective cosmological constant during inflation by
virtue of a quasi-de Sitter evolution and shows that the vacuum energy
contribution can manifest as \emph{geometric particles} produced by inflaton
fluctuations, with particular emphasis on super-Hubble modes. We conjecture
these particles as \emph{quasi-particles} arising from interaction between the
inflaton and spacetime geometry, enhanced by non-minimal coupling.
Specifically, we propose that dark matter arises from a pure geometric
quasi-particle contribution, and we quantify the corresponding dark matter
candidate ranges of mass. In this scenario, we further find that a zero
potential offset leads to a bare cosmological constant at the end of inflation,
while a negative offset would require an additional kinetic (or potential)
contribution in order to be fully-canceled. In this regard, we conclude that
the scenario of large field inflaton is preferred since it necessitates a more
appropriate selection of the offset. Our conclusion is reinforced as small
field inflaton would lead to a significant screening of the Newtonian
gravitational constant as inflation ends.

General Relativity and Quantum Cosmology;Cosmology and Nongalactic Astrophysics