  SNR G24.7+0.6 is a 9.5 kyrs radio and $\gamma$-ray supernova remnant evolving
in a dense medium. In the GeV regime, SNR G24.7+0.6
(3FHL\,J1834.1--0706e/FGES\,J1834.1--0706) shows a hard spectral index
($\Gamma$$\sim$2) up to $200$\,GeV, which makes it a good candidate to be
observed with Cherenkov telescopes such as MAGIC. We observed the field of view
of \snr\ with the MAGIC telescopes for a total of 31 hours. We detect very high
energy $\gamma$-ray emission from an extended source located 0.34\degr\ away
from the center of the radio SNR. The new source, named \mgc\ is detected up to
5\,TeV, and its spectrum is well-represented by a power-law function with
spectral index of $2.74 \pm 0.08$. The complexity of the region makes the
identification of the origin of the very-high energy emission difficult,
however the spectral agreement with the LAT source and overlapping position at
less than 1.5$\sigma$ point to a common origin. We analysed 8 years of
\fermi-LAT data to extend the spectrum of the source down to 60\,MeV.
\fermi-LAT and MAGIC spectra overlap within errors and the global broad band
spectrum is described by a power-law with exponential cutoff at
$1.9\pm0.5$\,TeV. The detected $\gamma$-ray emission can be interpreted as the
results of proton-proton interaction between the supernova and the CO-rich
surrounding.
