Context : Young massive clusters are usually deeply embedded in dust and gas .
They represent perfect astrophysical laboratories for study of massive stars .
Clusters with Wolf-Rayet ( WR ) stars are of special importance , since this enables us to study a coeval WR population at a uniform metallicity and known age .

Aims : We started a long-term project to search the inner Milky Way for hidden star clusters and to study them in details .
GLIMPSE 30 ( G30 ) is one of them .
The cluster is situated near the Galactic plane ( l =298 \aas@@fstack { \circ } 756 , b = - 0 \aas@@fstack { \circ } 408 ) and we aimed to determine its physical parameters and to investigate its high-mass stellar content and especially WR stars .

Methods : Our analysis is based on SOFI/NTT J _ { S } HK _ { S } imaging and low resolution ( R \sim 2000 ) spectroscopy of the brightest cluster members in the K atmospheric window .
For the age determination we applied isochrone fits for MS and Pre-MS stars .
We derived stellar parameters of the WR stars candidates using a full nonLTE modeling of the observed spectra .

Results : Using a variety of techniques we found that G30 is very young cluster , with age t \approx 4 Myr .
The cluster is located in Carina spiral arm , it is deeply embedded in dust and suffers reddening of A _ { V } \sim 10.5 \pm 1.1 mag .
The distance to the object is d=7.2 \pm 0.9 kpc .
The mass of the cluster members down to 2.35 \cal M _ { \odot } is \sim 1600 \cal M _ { \odot } .
Cluster ’ s MF for the mass range of 5.6 to 31.6 { \cal M _ { \odot } } shows a slope of \Gamma = -1.01 \pm 0.03 .
The total mass of the cluster obtained by this MF down to 1 \cal M _ { \odot } is about 3 \times 10 ^ { 3 } \cal M _ { \odot } .
The spectral analysis and the models allow us to conclude that in G30 are at least one Ofpe/WN and two WR stars .
The WR stars are of WN6-7 hydrogen rich type with progenitor masses more than 60 \cal M _ { \odot } .

Conclusions : G30 is a new member of the exquisite family of young Galactic clusters , hosting WR stars .
It is a factor of two to three less massive than some of the youngest super-massive star clusters like Arches , Quintuplet and Central cluster and is their smaller analog .