  The study of stripped-envelope core-collapse supernovae (SNe), with evidence
for strong interaction of SN ejecta with the circumstellar medium (CSM),
provides insights into the pre-supernova progenitor, and a fast-forwarded view
of the progenitor mass-loss history. In this context, we present late-time
radio observations of SN2004dk, a type Ibc supernova located in the galaxy, NGC
6118, at a distance of $d_L \approx 23$ Mpc. About 15 years after explosion,
SN2004dk has shown evidence for H$\alpha$ emission, possibly linked to the SN
ejecta interacting with an H-rich CSM. Using data from the VLA Low Band
Ionosphere and Transient Experiment (VLITE), we confirm the presence of a
late-time radio re-brightening accompanying the observed H$\alpha$ emission. We
model the SN2004dk radio light curves within the (spherically symmetric)
synchrotron-self-absorption (SSA) model. Within this model, our VLITE
observations combined with previously collected VLA data favor an
interpretation of SN2004dk as a strongly CSM-interacting radio SN going through
a complex environment shaped by a non-steady mass-loss from the SN progenitor.
