Publications with atmospheric pressure data on Mars are rather scarce.
This publication about seasonal cycles at Gale Crater shows the chart below with the atmospheric pressure ranges near the landing site of the Mars rover Curiosity.
The width of the band is an indication of how the pressure varies throughout each sol. The seasonal ups and downs show a known global pattern on Mars that illustrates another way the Red Planet differs from Earth. Most of the thin Martian atmosphere is carbon dioxide. Some of the carbon dioxide freezes out of the atmosphere into seasonal polar caps of carbon-dioxide ice. The biggest dips in the blue band are in the long southern-hemisphere winters - the result of carbon dioxide temporarily shifting out of the atmosphere into Mars' south polar ice cap. The dip in southern summer, less dramatic, results from carbon dioxide being captured temporarily into the less-massive north polar ice cap.
From the image above we can see that the pressure varies between about 6.9 and 9.7 millibars at Gale Crater, the difference between highest and lowest is thus 29% of the highest value.
This paper about the Viking mission mentions that the mean daily pressure observed by the Viking Lander 1 was as low as 6.8 millibars, at other times of the year it was as high as 9.0 millibars.
Here the difference between highest and lowest is thus almost 25% of the highest value.
The pressures at the Viking Lander 2 site were as low as 7.3 millibars and as high as 10.8 millibars, giving even a difference of almost 33% of the highest value !
If we assume that the pressure of 12.4 millibars at Hellas Planitia is the highest and considering that the difference between lowest and highest pressure will be no more than one third of the 12.4 millibars, the lowest pressure at Hellas Planitia will still be more than 8 millibars !
And because so far cyclones at Hellas Planitia have never been recorded, we don't have to expect low pressure eyes.