  The requirement of intermediate line component in the recently observed
spectra of several AGNs points to possibility of the existence of a physically
separate region between broad line region (BLR) and narrow line region (NLR).
In this paper we explore the emission from intermediate line region (ILR) by
using the photoionization simulations of the gas clouds distributed radially
from the AGN center. The gas clouds span distances typical for BLR, ILR and
NLR, and the appearance of dust at the sublimation radius is fully taken into
account in our model. Single cloud structure is calculated under the assumption
of the constant pressure. We show that the slope of the power law cloud density
radial profile does not affect the existence of ILR in major types of AGN. We
found that the low ionization iron line, Fe~II, appears to be highly sensitive
for the presence of dust and therefore becomes potential tracer of dust content
in line emitting regions. We show that the use of disk-like cloud density
profile computed at the upper part of the accretion disc atmosphere reproduces
the observed properties of the line emissivities. In particular, the distance
of H${\beta}$ line inferred from our model agrees with that obtained from the
reverberation mapping studies in Sy1 galaxy NGC 5548.
