After spending almost a decade in a radio-quiet state, the Anomalous X-ray Pulsar XTEJ1810–197 turned back on in early December 2018. We have observed this radio magnetar at 1.5 GHz with∼daily cadence since the ﬁrst detection of radio re-activation on 8 December 2018. In this paper, we report on the current timing properties of XTEJ1810–197 and ﬁnd that the magnitude of the spin frequency derivative has increased by a factor of 2.6 over our 48-day data set. We compare our results with the spin-down evolution reported during its previous active phase in the radio band. We also present total intensity pulse proﬁles at ﬁve diﬀerent observing frequencies between 1.5 and 8.4 GHz, collected with the Lovell and the Eﬀelsberg telescopes. The proﬁle evolution in our data set is less erratic than what was reported during the previous active phase, and can be seen varying smoothly between observations. Proﬁles observed immediately after the outburst show the presence of at least ﬁve cycles of a very stable ∼50-ms periodicity in the main pulse component that lasts for at least tens of days. This remarkable structure is seen across the full range of observing frequencies.