  We present a spatially-resolved study of the ionised gas in the central 2 kpc
of the Seyfert 2 galaxy NGC 2110 and investigate the role of its moderate
luminosity radio jet (kinetic radio power of $P_\mathrm{jet} = 2.3 \times
10^{43}\mathrm{erg\ s^{-1}}$). We use new optical integral-field observations
taken with the MEGARA spectrograph at GTC. We fit the emission lines with a
maximum of two Gaussian components, except at the AGN position where we used
three. Aided by existing stellar kinematics, we use the observed velocity and
velocity dispersion of the emission lines to classify the different kinematic
components. The disc component is characterised by lines with $\sigma \sim
60-200\ \mathrm{km\ s^{-1}}$. The outflow component has typical values of
$\sigma \sim 700\ \mathrm{km\ s^{-1}}$ and is confined to the central 400 pc,
which is coincident with linear part of the radio jet detected in NGC 2110. At
the AGN position, the [O III]$\lambda$5007 line shows high velocity components
reaching at least $1000\ \mathrm{km\ s^{-1}}$. This and the high velocity
dispersions indicate the presence of outflowing gas outside the galaxy plane.
Spatially-resolved diagnostic diagrams reveal mostly LI(N)ER-like excitation in
the outflow and some regions in the disc, which could be due to the presence of
shocks. However, there is also Seyfert-like excitation beyond the bending of
the radio jet, probably tracing the edge of the ionisation cone that intercepts
with the disc of the galaxy. NGC 2110 follows well the observational trends
between the outflow properties and the jet radio power found for a few nearby
Seyfert galaxies. All these pieces of information suggest that part of observed
ionised outflow in NGC 2110 might be driven by the radio jet. However, the
radio jet was bent at radial distances of 200 pc (in projection) from the AGN,
and beyond there, most of the gas in the galaxy disc is rotating.
