Type Ia supernova (SN Ia) light curves have a secondary maximum that exists in the r, i, and near-infrared filters. The secondary maximum is relatively weak in the r band, but holds the advantage that it is accessible, even at high redshift. We used Gaussian process fitting to parameterise the light curves of 893 SNe Ia from the Zwicky Transient Facility’s (ZTF) second data release (DR2), and we were able to extract information about the timing and strength of the secondary maximum. We found > 5σ correlations between the light curve dec rate (Δm15(g)) and the timing and strength of the secondary maximum in the r band. Whilst the timing of the secondary maximum in the i band is also correlated with Δm15(g), the strength of the secondary maximum in the i band shows significant scatter as a function of Δm15(g). We found that the transparency timescales of 97 per cent of our sample are consistent with double detonation models and that SNe Ia with small transparency timescales (< 32 d) reside predominantly in locally red environments. We measured the total ejected mass for the normal SNe Ia in our sample using two methods and both were consistent with medians of 1.3  ±  0.3 and 1.2  ±  0.2 M⊙. We find that the strength of the secondary maximum is a better standardisation parameter than the SALT light curve stretch (x1). Finally, we identified a spectral feature in the r band as Fe II, which strengthens during the onset of the secondary maximum. The same feature begins to strengthen at < 3 d post maximum light in 91bg-like SNe. Finally, the correlation between x1 and the strength of the secondary maximum was best fit with a broken, with a split at x10  =   − 0.5  ±  0.2, suggestive of the existence of two populations of SNe Ia.