  We present a 3D radiative transfer model for the Spectral Energy Distribution
(SED) of NGC 1365, which is a "changing look" Seyfert 1.8 type AGN. The SED
from the ultraviolet (UV) to the infrared (IR) is constructed using archival
data from the UVIT on-board $AstroSat$, along with IR data from the literature.
The SKIRT radiative transfer code is used to model the SED and derive the
geometry and composition of dust in this AGN. Similar to our earlier SED model
of NGC 4151, the nuclear region of NGC 1365 is assumed to contain a ring or
disk-like structure concentric to the accretion disk, composed of large
(0.1$\mu$m - 1$\mu$m) graphite grains in addition to the two-phase dusty torus
made up of ISM-type grains (Ring And Torus or RAT model). We also include, for
the first time, an additional component of dusty wind in the form of a bipolar
cone. We carry out a detailed analysis and derive the best-fit parameters from
a $\chi^2 $ test to be $R_{\rm in,r}$ = 0.03 pc, $\sigma$ = 26$^\circ$ and
$\tau$ = 20 for the assumed ring-torus-polar wind geometry. Our results suggest
the presence of hot dust at a temperature T $\sim$ 1216 K at the location of
the ring which absorbs and scatters the incident UV radiation and emits in the
near-IR (NIR). In the mid-IR (MIR) the major contributors are the polar cone
and warm dust with T $\sim$ 916 K at $R_{\rm in,t}$ = 0.1 pc. Not only are our
model radii in agreement with IR interferometric observations, our study also
reiterates the role of high resolution UV observations in constraining the dust
grain size distribution in the nuclear regions of AGN.
