  Recently, it has been realized that the so-called G-inflation model inspired
by supplementing a generalized covariant Galileon-like non-linear derivative
self-interacting term to the standard kinetic term should be ruled out from
inflationary models. This is due to the fact that it suffers from lack of an
oscillatory phase at the end of the inflationary regime which is typically
accompanied by the appearance of a negative squared propagation speed of the
scalar mode leading to instabilities of small-scale perturbations. In this
regard, the warm G-inflation scenario is proposed where for G-inflation to
survive, the Galileon scalar field is coupled to the radiation field through a
dissipation term which results in removing the reheating period due to the
characteristics of warm inflationary scenario. In so doing, a linear stability
analysis is first performed to obtain the appropriate slow-roll conditions in
such a proposal. Cosmological perturbations of the model are then investigated
by utilizing fluctuation-dissipation theorem and analytical expressions are
derived for observable quantities; the power spectrum, tilt spectral index and
tensor-to-scalar ratio in terms of $PSR$ parameters and Galileon flow
functions. Finally, the model is solved for chaotic self-interacting
potentials, particularly the renormalizable Higgs potential $\frac{\lambda}{4}
\phi^{4}$, and shown to be consistent with observations in the weak dissipation
$Q \ll 1+ 3\frac{\delta_{GX}}{\delta_{X}}$ and G-dominant
$3\frac{\delta_{GX}}{\delta_{X}}\gg 1$ regime despite its large self-coupling,
since the energy scale at the horizon crossing is depressed by the synergy of
Galileon and thermal effects.
