Context : The star formation process requires the dust and gas present in the Milky Way to self-assemble into dense reservoirs of neutral material where the new generation of stars will emerge .
Star-forming regions are usually studied in the context of Galactic surveys , but dedicated observations are sometimes needed when the study reaches beyond the survey area .

Aims : A better understanding of the star formation process in the Galaxy can be obtained by studying several regions .
This allows increasing the sample of objects ( clumps , cores , and stars ) for further statistical works and deeper follow-up studies .
Here , we studied the G345.5+1.5 region , which is located slightly above the Galactic plane , to understand its star formation properties .

Methods : We combined the Large Apex BOlometer CAmera ( LABOCA ) and ^ { 12 } CO ( 4 - 3 ) transition line ( NANTEN2 ) observations complemented with the Hi-GAL and \it { Spitzer } -GLIMPSE surveys to study the star formation toward this region .
We used the Clumpfind algorithm to extract the clumps from the 870 \mu m and ^ { 12 } CO ( 4 - 3 ) data .
Radio emission at 36 cm was used to estimate the number of H ii regions and to remove the contamination from the free-free emission at 870 \mu m. We employed color-color diagrams and spectral energy distribution ( SED ) slopes to distinguish between prestellar and protostellar clumps .
We studied the boundedness of the clumps through the virial parameter .
Finally , we estimated the star formation efficiency ( SFE ) and star formation rate ( SFR ) of the region and used the Schmidt-Kennicutt diagram to compare its ability to form stars with other regions of the Galactic plane .

Results : Of the 13 radio sources that we found using the MGPS-2 catalog , 7 are found to be associated with H ii regions corresponding to late-B or early-O stars .
We found 45 870 \mu m clumps with diameters between 0.4 and 1.2 pc and masses between 43 M _ { \sun } and 3923 M _ { \sun } , and 107 ^ { 12 } CO clumps with diameters between 0.4 pc and 1.3 pc and masses between 28 M _ { \odot } and 9433 M _ { \odot } .
More than 50 % of the clumps are protostellar and bounded and are able to host ( massive ) star formation .
High SFR and SFR density ( \Sigma _ { SFR } ) values are associated with the region , with an SFE of a few percent .

Conclusions : With submillimeter , CO transition , and short-wavelength infrared observations , our study reveals a population of massive stars , protostellar and bound starless clumps , toward G345.5+1.5 .
This region is therefore actively forming stars , and its location in the starburst quadrant of the Schmidt-Kennicutt diagram is comparable to other star-forming regions found within the Galactic plane .