Context :

Aims : The aim of this work is to investigate the characteristics of the young stellar population in the spiral galaxy NGC 247 .
In particular , we focused our attention in its hierarchical clustering distributions and the properties of the smallest groups .

Methods : We used multiband Hubble Space Telescope ( HST ) data from three fields covering more than half of NGC 247 to select the young population .
Then , through the path linkage criterion ( PLC ) , we found compact young star groups , and estimated their fundamental parameters , such as their stellar densities , sizes , amount of members and luminosity function ( LF ) slopes .
We also performed a fractal analysis to determinate the clustering properties of this population .
We build a stellar density map and the corresponding dendrograms corresponding to the galactic young population to detect large structures and draw their main characteristics .

Results : We detected 339 young star groups , for which we computed a mean radius of \sim 60 pc and a maximum in the size distribution between 30 and 70 pc .
We also obtained LF slopes with a bimodal distribution showing peaks at \sim 0.1 and \sim 0.2 .
We identified several candidates to HII regions which follow an excellent spatial correlation with the young groups found by the PLC .
We observed that the young population are hierarchically organized , where the smaller and denser structures are within larger and less dense ones .
We noticed that all these groups presented a fractal subclustering , following the hierarchical distribution observed in the corresponding stellar density map .
For the large young structures observed in this map , we obtained a fractal dimension of \sim 1.6-1.8 using the perimeter-area relation and the cumulative size distribution .
These values are consistent with a scenario of hierarchical star formation .

Conclusions :