  AD Leo is a young and active M dwarf with high flaring rates across the X-ray
to radio bands. Flares accelerate particles in the outer coronal layers and
often impact exospace weather. Wide-band radio dynamic spectra let us explore
the evolution of particle acceleration activity across the corona. Identifying
the emission features and modelling the mechanisms can provide insights into
the possible physical scenarios driving the particle acceleration processes. We
performed an 8 h monitoring of AD Leo across the 550 - 850 MHz band using
upgraded-Giant Metrewave Radio Telescope (uGMRT). A python routine, named
VISAD, was built to obtain the visibility averaged wide-band dynamic spectra.
Direct imaging was also performed. Based on existing observational results on
AD Leo and on solar active region models, radial profiles of electron density
and magnetic fields were derived. Applying these models, we explore the
possible emission mechanisms and magnetic field structure of the active region.
The star displayed high brightness temperature ($\approx 10^{10} - 10^{11}$ K)
throughout the observation with nearly 100% left circularly polarised bursts.
Post flare phase is characterised by a highly polarised (60 - 80%) solar-like
type IV burst confined above 700 MHz.The flare emission favors a Z-mode or a
higher harmonic X-mode electron cyclotron maser emission mechanism. The
post-flare activity above 700 MHz is consistent with a type-IV radio burst from
flare-accelerated particles trapped in magnetic loops, which could be a coronal
mass ejection (CME) signature. This is the first solar-like type-IV burst
reported on a young active M dwarf belonging to a different age - related
activity compared to the Sun. We also find that, a multipole expansion model of
the active region magnetic field better accounts for the observed radio
emission than a solar-like active region profile.
