jats:pGravitational instability is thought to be one of the main drivers of angular momentum transport in young protoplanetary discs. The disc around Elias 2−27 offers a unique example of gravitational instability at work. It is young and massive, displaying two prominent spiral arms in dust continuum emission and global non-axisymmetric kinematic signatures in molecular line data. In this work, we used archival ALMA observations of jats:sup13</jats:sup>CO line emission to measure the efficiency of angular momentum transport in the Elias 2−27 system through the kinematic signatures generated by gravitational instability, known as “GI wiggles”. Assuming the angular momentum is transported by the observed spiral structure and leveraging previously-derived dynamical disc mass measurements, the amount of angular momentum transport we found corresponds to an jats:italicα</jats:italic>-viscosity of jats:italicα</jats:italic> = 0.038 ± 0.018. This value implies an accretion rate onto the central star of logjats:sub10</jats:sub> jats:italicṀ</jats:italic>jats:sub⋆</jats:sub> = −6.99 ± 0.17 jats:italicM</jats:italic>jats:sub⊙</jats:sub> yrjats:sup−1</jats:sup>, which reproduces the one observed value of logjats:sub10</jats:sub> jats:italicṀ</jats:italic>jats:sub⋆,obs</jats:sub> = −7.2 ± 0.5 jats:italicM</jats:italic>jats:sub⊙</jats:sub> yrjats:sup−1</jats:sup> very well. The excellent agreement we have found serves as further proof that gravitational instability is the main driver of angular momentum transport acting in this system.</jats:p>