  Black hole driven outflows in galaxies hosting active galactic nuclei (AGN)
may interact with their interstellar medium (ISM) affecting star formation.
Such feedback processes, reminiscent of those seen in massive galaxies, have
been reported recently in some dwarf galaxies. However, such studies have
usually been on kiloparsec and larger scales and our knowledge on the smallest
spatial scales to which these feedback processes can operate is unclear. Here
we demonstrate radio jet$-$ISM interaction on the scale of an asymmetric triple
radio structure of $\sim$ 10 parsec size in NGC 4395. This triple radio
structure is seen in the 15 GHz continuum image and the two asymmetric jet-like
structures are situated on either side of the radio core that coincides with
the optical {\it Gaia} position. The high resolution radio image and the
extended [OIII]$\lambda$5007 emission, indicative of an outflow, are spatially
coincident and are consistent with the interpretation of a low power radio jet
interacting with the ISM. Modelling of the spectral lines using {\tt MAPPINGS},
and estimation of temperature using optical integral field spectroscopic data
suggest shock ionization of the gas. The continuum emission at 237 GHz, though
weak, was found to spatially coincide with the AGN. However, the CO(2$-$1) line
emission was found to be displaced by around 20 parsec northward of the AGN
core. The spatial coincidence of molecular H$_2$$\lambda$2.4085 along the jet
direction, the morphology of ionised [OIII]$\lambda$5007 and displacement of
the CO(2$-$1) emission argues for conditions less favourable for star formation
in the central $\sim$ 10 parsec region.
