  (Abridged) Exoplanetary research has provided us with exciting discoveries of
planets around very low-mass (VLM) stars (e.g., TRAPPIST-1 and Proxima
Centauri). However, current theoretical models strive to explain planet
formation in these conditions and do not predict the development of giant
planets. Recent high-resolution observations from ALMA of the disk around CIDA
1, a VLM star in Taurus, show substructures hinting at the presence of a
massive planet. We aim to reproduce the dust ring of CIDA 1, observed in the
dust continuum emission in ALMA Band 7 (0.9 mm) and Band 4 (2.1 mm), along with
its $^{12}$CO (J=3-2) and $^{13}$CO (J=3-2) channel maps, assuming the
structures are shaped by the interaction of the disk with a massive planet. We
seek to retrieve the mass and position of the putative planet. We model the
protoplanetary disk with a set of hydrodynamical simulations, varying the mass
and locations of the embedded planet. We compute the dust and gas emission
using radiative transfer simulations, and, finally, we obtain the synthetic
observations treating the images as the actual ALMA observations. Our models
indicate that a planet with a minimum mass of $\sim1.4\,\text{M}_\text{Jup}$
orbiting at a distance of $\sim 9-10$ au can explain the morphology and
location of the observed dust ring at Band 7 and Band 4. We can reproduce the
low spectral index ($\sim 2$) observed where the dust ring is detected. Our
synthetic images reproduce the morphology of the $^{12}$CO and $^{13}$CO
observed channel maps where the cloud absorption allowed a detection. Applying
an empirical relation between planet mass and gap width in the dust, we predict
a maximum planet mass of $\sim4 - 8\,\text{M}_\text{Jup}$. Our results suggest
the presence of a massive planet orbiting CIDA 1, thus challenging our
understanding of planet formation around VLM stars.
