  We compute the non-thermal emissions produced by relativistic particles
accelerated by the AGN-driven shocks in NGC 1068, and we compare the model
predictions with the observed gamma-ray and radio spectra . The former is
contributed by pion decay, inverse Compton scattering, and bremsstrahlung,
while the latter is produced by synchrotron radiation. We derive the gamma-ray
and radio emissions by assuming the standard acceleration theory, and we
discuss how our results compare with those corresponding to other commonly
assumed sources of gamma-ray and radio emissions, like Supernova remnants (SNR)
or AGN jets. We find that the AGN-driven shocks observed in the circumnuclear
molecular disk of such a galaxy provide a contribution to the gamma-ray
emission comparable to that provided by the starburst activity when standard
particle acceleration efficiencies are assumed, while they can yield the whole
gamma-ray emission only when the parameters describing the acceleration
efficiency and the proton coupling with the molecular gas are tuned to values
larger than those assumed in standard, SNR-driven shocks. We discuss the range
of acceleration efficiencies (for protons and electrons) and of proton
calorimetric fractions required to account for the observed gamma-ray emission
in the AGN outflow model. We further compare the neutrino flux expected in our
model with constraints from current experiments, and we provide predictions for
the detections by the upcoming KM3NeT neutrino telescope. This analysis
strongly motivates observations of NGC 1068 at >TeV energies with current and
future Cherenkov telescopes in order to gain insight into the nature of the
gamma-rays source.
