  This study presents a detailed analysis of the GAL045.804-0.356 massive
star-forming clump. A high-angular resolution and sensitivity observations were
conducted using MeerKAT at 1.28 GHz and ALMA interferometer at 1.3 mm. Two
distinct centimetre radio continuum emissions (source A and source B) were
identified within the clump. A comprehensive investigation was carried out on
source A, the G45.804-0.355 star-forming region (SFR) due to its association
with Extended Green Object (EGO), 6.7 GHz methanol maser and the spatial
coincidence with the peak of the dust continuum emission at 870 $\mu$m. The
ALMA observations revealed seven dense dust condensations (MM1 to MM7) in
source A. The brightest ($S_{\rm \nu} \sim$ 87 mJy) and massive main dense
core, MM1, was co-located with the 6.7 GHz methanol maser. Explorations into
the kinematics revealed gas motions characterised by a velocity gradient across
the MM1 core. Furthermore, molecular line emission showed the presence of an
extended arm-like structure, with a physical size of 0.25 pc $\times$ 0.18 pc
($\sim$ 50000 au $\times$ 30000 au) at a distance of 7.3 kpc. Amongst these
arms, two arms were prominently identified in both the dust continuum and some
of the molecular lines. A blue-shifted absorption P-Cygni profile was seen in
the H$_2$CO line spectrum. The findings of this study are both intriguing and
new, utilising data from MeerKAT and ALMA to investigate the characteristics of
the AGAL45 clump. The evidence of spiral arms, the compact nature of the EGO
and $<$ 2 km s$^{-1}$ velocity gradient are all indicative of G45.804-0.355
being oriented face-on.
