Optical observations of the type IIb SN 2013df from a few days to about 250 days after explosion are presented. These observations are complemented with UV photometry taken by \textit{SWIFT} up to 60 days post-explosion. The double-peak optical light curve is similar to those of SNe 1993J and 2011fu although with different decline and rise rates. From the modelling of the bolometric light curve, we have estimated that the total mass of synthesised $^{56}$Ni in the explosion is $∼0.1$ M$_{⊙}$, while the ejecta mass is $0.8-1.4$ M$_{⊙}$ and the explosion energy $0.4-1.2 \times 10^{51}$erg. In addition, we have estimated a lower limit to the progenitor radius ranging from $64-169$ $R_{⊙}$. The spectral evolution indicates that SN 2013df had a hydrogen envelope similar to SN 1993J ($∼ 0.2$ M$_{⊙}$). The line profiles in nebular spectra suggest that the explosion was asymmetric with the presence of clumps in the ejecta, while the [O\,{\sc i}] $λ$λ$6300$, $6364$ luminosities, may indicate that the progenitor of SN 2013df was a relatively low mass star ( $∼ 12-13 $ M$_{⊙}$). ; Comment: 18 pages, 11 figures, 9 tables, accepted for publication in MNRAS