Abstract Dust traps are the most promising mechanisms to explain the observed substructures in protoplanetary discs. In this work, we present high-angular resolution (∼60 mas, 9.4 au) and high-sensitivity Atacama Large Millimetre/submillimetre Array (ALMA) observations at 3 mm of the transitional disc around LkCa15. The new data, combined with previous high-resolution observations at λ = 0.87, 1.3 mm, make LkCa15 an ideal laboratory for testing the dust trapping mechanism. We found that the width of the three rings decreases linearly with frequency, and the spectral indices show local minima at the locations of the rings, consistent with dust trap models. Multi-wavelength modelling confirms that the dust surface density and maximum grain size peak at 69 and 101 au, and suggestive peak at 42 au. The estimated total dust mass is between 13-250 M⊕, depending on the chosen opacity. The inner disc shows bright and unresolved emission at 3 mm, exhibiting a spectral index of $\alpha _{1.3-3 \rm mm} = 0.3 \pm 0.37$, and α3mm-3cm ranging from −0.1 to 0.0. These properties are consistent with free-free emission from an ionised jet or disc wind. Dust evolution models and radiative transfer calculations suggest that a viscosity coefficient of α = 10−3, a fragmentation velocity of 10 m s−1, and DSHARP opacities provide the best match to the observed properties.