  HESS J1809-193 is an unidentified TeV source, first detected by the High
Energy Stereoscopic System (H.E.S.S.) Collaboration. The emission originates in
a source-rich region that includes several Supernova Remnants (SNR) and Pulsars
(PSR) including SNR G11.1+0.1, SNR G11.0-0.0, and the young radio pulsar
J1809-1917. Originally classified as a pulsar wind nebula (PWN) candidate,
recent studies show the peak of the TeV region overlapping with a system of
molecular clouds. This resulted in the revision of the original leptonic
scenario to look for alternate hadronic scenarios. Marked as a potential
PeVatron candidate, this region has been studied extensively by H.E.S.S. due to
its emission extending up-to several tens of TeV. In this work, we use 2398
days of data from the High Altitude Water Cherenkov (HAWC) observatory to carry
out a systematic source search for the HESS J1809-193 region. We were able to
resolve emission detected as an extended component (modelled as a Symmetric
Gaussian with a 1 $\sigma$ radius of 0.21 $^\circ$) with no clear cutoff at
high energies and emitting photons up-to 210 TeV. We model the multi-wavelength
observations for the region HESS J1809-193 using a time-dependent leptonic
model and a lepto-hadronic model. Our model indicates that both scenarios could
explain the observed data within the region of HESS J1809-193.
