  NGC 4330 is one of the Virgo galaxies whose UV distribution shows a tail
structure. An associated tail structure is also observed in the HI and
H$\alpha$ emission distributions. Previous dynamical modeling showed that the
galaxy is approaching the cluster center and is therefore undergoing increasing
ram pressure stripping. Recent stellar population fitting of deep optical
spectra together with multiband photometry lead to the determination of the
time when star formation was quenched in the galactic disk. We introduce a new
version of the dynamical model that includes the diffuse ionized gas and aim to
reproduce the HI, H$\alpha$, UV distributions together with the star formation
histories of the outer gas-free parts of the galactic disk. The results of 50
simulations with five different Lorentzian temporal ram-pressure profiles and
five different delays between the simulation onset and peak ram pressure are
presented. The inclusion of diffuse gas stripping changes significantly the HI,
UV, and H$\alpha$ emission distributions. The simulations with diffuse gas
stripping naturally lead to vertical low surface density filaments in the
downwind region of the galactic disk. These filaments occur less frequently in
the simulations without diffuse gas stripping. The simulations with diffuse gas
stripping lead to better joint fits to the SEDs and optical spectra. The HI,
NUV, and H$\alpha$ morphologies of the model snapshots which best reproduce the
SEDs and optical spectra are sufficiently different to permit a selection of
best-fit models. We conclude that the inclusion of diffuse gas stripping
significantly improves the resemblance between the model and observations. Our
preferred model yields a time to peak ram pressure of 140 Myr in the future.
The spatial coincidence of the radio continuum and diffuse H$\alpha$ tails
suggests that both gas phases are stripped together.
