  We model the energetic storm particle (ESP) event of 14 July 2012 using the
energetic particle acceleration and transport model named PARADISE, together
with the solar wind and coronal mass ejection (CME) model named EUHFORIA. The
simulation results illustrate both the capabilities and limitations of the
utilised models. We show that the models capture some essential structural
features of the ESP event; however, for some aspects the simulations and
observations diverge. We describe and, to some extent, assess the sources of
errors in the modelling chain of EUHFORIA and PARADISE and discuss how they may
be mitigated in the future. The PARADISE model evolves energetic particle
distributions in a background solar wind generated by the ideal MHD module of
EUHFORIA. The CME generating the ESP event is simulated by using the spheromak
model of EUHFORIA, which approximates the CME's flux rope as a linear
force-free spheroidal magnetic field. In addition, a tool was developed to
trace CME-driven shock waves in the EUHFORIA simulation domain. This tool is
used in PARADISE to (i) inject 50 keV protons continuously at the CME-driven
shock and (ii) include a foreshock and a sheath region, in which the energetic
particle parallel mean free path, $\lambda_\parallel$, decreases towards the
shock wave. The value of $\lambda_\parallel$ at the shock wave is estimated
from in situ observations of the ESP event. For energies below 1 MeV, the
simulation results agree well with both the upstream and downstream components
of the ESP event observed by the Advanced Composition Explorer (ACE). This
suggests that these low-energy protons are mainly the result of interplanetary
particle acceleration. In the downstream region, the sharp drop in the
energetic particle intensities is reproduced at the entry into the following
magnetic cloud, illustrating the importance of a magnetised CME model.
