  This is the second in a series of papers devoted to explore a set of six
dusty models of active galactic nuclei (AGN) with available spectral energy
distributions (SEDs). These models are the smooth torus by Fritz et al. (2006),
the clumpy torus by Nenkova et al. (2008B), the clumpy torus by Hoenig &
Kishimoto (2010), the two phase torus by Siebenmorgen et al. (2015), the two
phase torus by Stalevski et al. (2016), and the wind model by Hoenig &
Kishimoto (2017). The first paper explores discrimination among models and the
parameter restriction using synthetic spectra (Gonzalez-Martin et al. 2019A).
Here we perform spectral fitting of a sample of 110 AGN drawn from the
Swift/BAT survey with Spitzer/IRS spectroscopic data. The aim is to explore
which is the model that describes better the data and the resulting parameters.
The clumpy wind-disk model by Hoenig & Kishimoto (2017) provides good fits for
~50% of the sample, and the clumpy torus model by Nenkova et al. (2008B) is
good at describing ~30% of the objects. The wind-disk model by Hoenig &
Kishimoto (2017) is better for reproducing the mid-infrared spectra of Type-1
Seyferts while Type-2 Seyferts are equally fitted by both models. Large
residuals are found irrespective of the model used, indicating that the AGN
dust continuum emission is more complex than predicted by the models or that
the parameter space is not well sampled. We found that all the resulting
parameters for our AGN sample are roughly constrained to 10-20% of the
parameter space. The derived outer radius of the torus is smaller for the
smooth torus by Fritz et al. (2006) and the two phase torus by Stalevski et al.
(2016) than the one derived from the clumpy torus by (Nenkova et al. 2008B).
Covering factors and line-of-sight viewing angles strongly depend on the model
used. The total dust mass is the most robust derived quantity.
