  We present an analysis of the new, deep (94\,ksec) {\it Chandra} ACIS-S
observation of radio-loud active galaxy CGCG\,292$-$057, characterized by a
LINER-type nucleus and a complex radio structure that indicates intermittent
jet activity. On the scale of the host galaxy bulge, we detected excess X-ray
emission with a spectrum best fit by a thermal plasma model with a temperature
of $\sim 0.8$\,keV. We argue that this excess emission results from compression
and heating of the hot diffuse fraction of the interstellar medium displaced by
the expanding inner, $\sim 20$\, kpc-scale lobes observed in this restarted
radio galaxy. The nuclear X-ray spectrum of the target clearly displays an
ionized iron line at $\sim 6.7$\,keV, and is best fitted with a
phenomenological model consisting of a power-law (photon index $\simeq 1.8$)
continuum absorbed by a relatively large amount of cold matter (hydrogen column
density $\simeq 0.7 \times 10^{23}$\,cm$^{-2}$), and partly scattered (fraction
$\sim 3\%$) by ionized gas, giving rise to a soft excess component and
K$\alpha$ line from iron ions. We demonstrate that the observed X-ray spectrum,
particularly the equivalent width of Fe\,\texttt{XXV} K$\alpha$ (of order
$0.3$\,keV) can in principle, be explained in a scenario involving a
Compton-thin gas located at the scale of the broad-lined region in this source
and photoionized by nuclear illumination. We compare the general spectral
properties of the CGCG\,292$-$057 nucleus, with those of other nearby LINERs
studied in X-rays.
