Abstract <p>Collimated ejecta of matter, otherwise known as jets, are observed in large quantities in the chromosphere and lower corona of the Sun and are of great interest in relation to their possible role for the transport of matter and energy in the solar atmosphere. These jets are subdivided into several groups characterized by different formation mechanisms and substantial variation of their characteristics. In order to distinguish separate groups of jets and identify them with respective formation mechanisms, we performed a statistical analysis of the full ensemble of solar extreme ultraviolet (EUV) jets using observations from the Solar Dynamics Observatory (SDO) in the 171, 193, and 304 Å channels. We identified a total of 212 such events, of which 26% were classified as linear jets, probably generated by magnetoacoustic shocks, and 30% as helical jets, representing small-scale filament eruptions. We found that these two groups differ significantly in their major dynamic characteristics (maximum height, initial velocity, and lifetime), as well as in their widths that are closely related to the underlying magnetic field structure, while helical jets were also shown to be much more frequently associated with the presence of hot coronal component. At the same time, we found a third class of jets with intermediate characteristics and unknown formation mechanism, requiring further study.</p>